diff options
Diffstat (limited to 'fg21sim/extragalactic')
| -rw-r--r-- | fg21sim/extragalactic/clusters/halo.py | 50 |
1 files changed, 50 insertions, 0 deletions
diff --git a/fg21sim/extragalactic/clusters/halo.py b/fg21sim/extragalactic/clusters/halo.py index 2cc391f..b65cd08 100644 --- a/fg21sim/extragalactic/clusters/halo.py +++ b/fg21sim/extragalactic/clusters/halo.py @@ -254,6 +254,56 @@ class RadioHalo: emissivity = syncem.emissivity(frequencies) return emissivity + def calc_power(self, emissivity): + """ + Calculate the synchrotron power (i.e., power *emitted* per + unit frequency) from emissivity. + + NOTE + ---- + The calculated power (a.k.a. spectral luminosity) is in units of + [W/Hz] which is common in radio astronomy, instead of [erg/s/Hz]! + 1 [W] = 1e7 [erg/s] + + Parameters + ---------- + emissivity : float, or 1D `~numpy.ndarray` + The synchrotron emissivity at multiple frequencies. + Unit: [erg/s/cm^3/Hz] + + Returns + ------- + power : float, or 1D `~numpy.ndarray` + The calculated synchrotron power w.r.t. each input emissivity. + Unit: [W/Hz] + """ + emissivity = np.asarray(emissivity) + power = emissivity * self.volume # [erg/s/Hz] + power *= 1e-7 # [erg/s/Hz] -> [W/Hz] + return power + + def calc_flux(self, emissivity): + """ + Calculate the synchrotron flux density (i.e., power *observed* + per unit frequency) from emissivity. + + Parameters + ---------- + emissivity : float, or 1D `~numpy.ndarray` + The synchrotron emissivity at multiple frequencies. + Unit: [erg/s/cm^3/Hz] + + Returns + ------- + flux : float, or 1D `~numpy.ndarray` + The calculated synchrotron flux w.r.t. each input emissivity. + Unit: [Jy] = 1e-23 [erg/s/cm^2/Hz] = 1e-26 [W/m^2/Hz] + """ + power = self.calc_power(emissivity) # [W/Hz] + DL = COSMO.DL(self.z) * AUC.Mpc2m # [m] + flux = 1e26 * power / (4*np.pi * DL*DL) # [Jy] + return flux + def fp_injection(self, gamma, t=None): """ Electron injection (rate) term for the Fokker-Planck equation. |